Abrupt Longitudinal Magnetic Field Changes and Ultraviolet Emissions Accompanying Solar Flares

TL;DR

This study compares UV emissions and magnetic field changes during four X-class solar flares, revealing that UV emissions generally precede magnetic field changes and are spatially coincident with them, supporting a wave propagation model.

Contribution

It provides observational evidence linking UV emissions and magnetic field changes during solar flares, highlighting the timing and spatial relationships that support a wave propagation mechanism.

Findings

UV emissions lead magnetic field changes by 4-9 minutes on average.

Magnetic field changes are significant, abrupt, and persistent across multiple pixels.

UV emissions continue for tens of minutes after magnetic field changes are complete.

Abstract

We have used Transition Region and Coronal Explorer (TRACE) 1600 \AA images and Global Oscillation Network Group (GONG) magnetograms to compare ultraviolet (UV) emissions from the chromosphere to longitudinal magnetic field changes in the photosphere during four X-class solar flares. An abrupt, significant, and persistent change in the magnetic field occurred across more than ten pixels in the GONG magnetograms for each flare. These magnetic changes lagged the GOES flare start times in all cases, showing that they were consequences and not causes of the flares. Ultraviolet emissions were spatially coincident with the field changes. The UV emissions tended to lag the GOES start times for the flares, and led the changes in the magnetic field in all pixels except one. The UV emissions led the photospheric field changes by 4 minutes on average with the longest lead being 9 minutes, however, the UV emissions continued for tens of minutes, and more than an hour in some cases, after the field changes were complete. The observations are consistent with the picture in which an Alfv\'{e}n wave from the field reconnection site in the corona propagates field changes outward in all directions near the onset of the impulsive phase, including downwards through the chromosphere and into the photosphere, causing the photospheric field changes, whereas the chromosphere emits in the UV in the form of flare kernels, ribbons and sequential chromospheric brightenings during all phases of the flare.